Neutron stars in modified teleparallel gravity

Vilhena, S. G.; Duarte, S. B.; Dutra, M.; Pompeia, P. J.

doi:10.1088/1475-7516/2023/04/044

Cited by 7 publications

(5 citation statements)

References 95 publications

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“…For isotropic fluid background i.e. for p r = p t , the TOV equation reformulated to simultaneous differential equation of mass and density in equations (48) and (49) and further reformulated in equations ( 50) and (51) for polytropic gas model background. From equations (50) and (51) mass and density has been evaluated with the boundary condition from table 3 and graphically represented.…”

Section: Discussionmentioning

confidence: 99%

“…In [94] a generic solution to the Einstein system in among of the gravitational potentials in spherically symmetric spacetime that models anisotropic strange quark matter by establishing the barotropic equation of state. Equations ( 22) and ( 23) has been reformulated for isotropic gas background in the form of equations (48) and (49). Now using barotropic Eos from equation (52) reconstructed pair of differential equation is…”

Section: Barotropic Gas Model Backgroundmentioning

confidence: 99%

“…Various modified gravity theory are f (R) theory [40,41], f (T) theory [42,43], f (G) theory [44,45], f (R, T) theory [46,47], and so on. Astronomy's new frontier is the study of compact stars against the backdrop of modified gravity [48,49]. f (R) gravity theory, which initially begins with a universal function of the Ricci scalar R in the gravitational action, is one of the most well-liked modified gravity theories.…”

Section: Introductionmentioning

confidence: 99%

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Realistic compact objects in the f(R, T) gravity in the background of polytropic and barotropic gas models

Das,

Chattopadhyay

2024

Phys. Scr.

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The $f(R,T)$ gravity in the background of the polytropic and barotropic fluid has been investigated in this work. We have selected the TOV equation to determine the internal spacetime of a spherically symmetric galactic object. With the use of the Einstein equation, we have selected KB-spacetime to calculate the mass, compactness, and surface redshift of a spherically symmetric body. Explicit conditions for model parameters have been constructed for the boundary conditions of the interior and exterior spacetime, and the Schwarzschild solution has been employed in the modified $f(R,T)$ gravity theory to evaluate different matching criteria. An increasing pattern in compactness with respect to the different radii is evident in the graphical representation of the compactness evolution for each of the individual star models. After selecting a non-vacuum field equation for \textcolor{red}{higher order curvature}, we reformulated $f(R,T)$ for $R$ and $T$. As a result, the tangential pressure, radial pressure, and matter density have all been calculated. According to the study, as the radius goes to infinity, the tangential and radial pressures display asymptotic flatness and converge to zero. Polytropic and barotropic gas EoS have been adopted since the star model confronts the presence of an isotropic fluid backdrop. It has been noted that in a polytropic background, both density and pressure increase with distance from the star's core, but in a barotropic background, the pressure exhibits an ascending pattern as a function of radius.

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Section: Discussionmentioning

confidence: 99%

Section: Barotropic Gas Model Backgroundmentioning

confidence: 99%

Section: Introductionmentioning

confidence: 99%

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Realistic compact objects in the f(R, T) gravity in the background of polytropic and barotropic gas models

Das,

Chattopadhyay

2024

Phys. Scr.

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“…At the same time, in the recent papers [18,19], people study the very same New GR theory using a very different approach. From the erroneous claim 7 that energy-momentum conservation requires a + b = 2c, they restricted the model parameters to only the ones which give precisely the same static spherically symmetric solutions as in GR.…”

Section: The Special Casesmentioning

confidence: 99%

Static spherically symmetric solutions in new general relativity

Golovnev,

Semenova,

Vandeev

2024

Class. Quantum Grav.

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We give a pedagogical introduction to static spherically symmetric solutions in models of New GR, both explaining the basics and showing how all such vacuum solutions can be obtained in elementary functions. In doing so, we coherently introduce the full landscape of these modified teleparallel spacetimes, and find a few special cases. The equations of motion are turned into a very nice and compact form by using the Levi-Civita divergence of the torsion-conjugate; and generalised Bianchi identities are briefly discussed. Another important point we make is that a convenient choice of the radial variable might be instrumental for success of similar studies in other modified gravity models.

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“…While in GR the argument of the integral action is the scalar curvature, in TEGR the argument is the scalar torsion (T), an object that is assembled as a linear combination of all independent quadratic invariants built with the torsion tensor. Similarly to what is done in the Riemann manifold, modified theories are also proposed with the replacement of the argument of the integral action by an arbitrary function of the scalar torsion, T → f (T) [34][35][36][37][38]. Although the equivalence of TEGR with GR is manifest, the same does not happen when we consider extensions like f (R) and f (T).…”

Section: Introductionmentioning

confidence: 99%

Second-order teleparallel gauge theory

Assencio,

Caraça,

Vilhena

et al. 2023

Class. Quantum Grav.

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In this work, we analyze second-order extensions of teleparallel theories of gravity as gauge theories for the translation group. We use Utiyama’s approach to gauge theories and show that it is possible to include second-order derivative terms in the Lagrangian of the gauge potential and preserve gauge invariance. Besides the usual field strength, a new object has to be introduced in order to preserve both gauge and diffeomorphism invariances. From this new object, we obtain a set of fourteen independent invariants which leads to equations that are linear in the fourth derivative of the tetrad field. We analyze a particular example with one of these invariants and evaluate the weak field limit, showing that the effective gravitational potential is a combination of Newton and Yukawa potentials.

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Neutron stars in modified teleparallel gravity

Cited by 7 publications

References 95 publications

Realistic compact objects in the f(R, T) gravity in the background of polytropic and barotropic gas models

Realistic compact objects in the f(R, T) gravity in the background of polytropic and barotropic gas models

Static spherically symmetric solutions in new general relativity

Second-order teleparallel gauge theory

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